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2-D velocity field structure and oscillations nearby quiescent filament

Published online by Cambridge University Press:  14 March 2005

G. P. Mashnich ,
V. S. Bashkirtsev ,
E. M. Golubeva ,
A. I. Khlystova  and
A. S. Letunov
G. P. Mashnich
Affiliation:
Institute of Solar-Terrestrial Physics, P.O. Box 4026, Irkutsk, Russia email: mashnich@iszf.irk.ru Present address: Institute of Solar-Terrestrial Physics, Lermontova, 126, Irkutsk, Russia
V. S. Bashkirtsev
Affiliation:
Institute of Solar-Terrestrial Physics, P.O. Box 4026, Irkutsk, Russia email: mashnich@iszf.irk.ru
E. M. Golubeva
Affiliation:
Institute of Solar-Terrestrial Physics, P.O. Box 4026, Irkutsk, Russia email: mashnich@iszf.irk.ru
A. I. Khlystova
Affiliation:
Institute of Solar-Terrestrial Physics, P.O. Box 4026, Irkutsk, Russia email: mashnich@iszf.irk.ru
A. S. Letunov
Affiliation:
Institute of Solar-Terrestrial Physics, P.O. Box 4026, Irkutsk, Russia email: mashnich@iszf.irk.ru
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Abstract

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We have developed the technique and software to observe and process spectral data obtained with the CCD camera. It makes possible to construct two-dimensional maps of Doppler velocity and intensity in solar features simultaneously at two levels in the solar atmosphere. We present some results derived from study of the structure and space-time variations of the Doppler velocity in the region of quiescent filaments in the chromosphere (the $H_{\beta}$$\lambda 486.1$ nm line) and under filaments in the photosphere (the Fe I $\lambda$ 486.3 nm. and Fe I $\lambda$ 485.9 nm lines). We came to a conclusion that motions in quiescent filaments consist of both the stationary and oscillatory components and follow helical trajectories.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 203 - 206
Copyright
© 2004 International Astronomical Union